, 1887-09-27
THE STAR OF BETHLEHEM.
Its History In Brief-A Popular FRus
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Its History In Brief-A Popular Fancy,
A Welcome Celestial Event.
"Where can the Star of Bethlehem be
found?' is the oft repeated question that
comes from many quarters. The fact is,
no such star is visible in any part of the
heavens. An observer with a vivid i'm
agination fancied he had discovered this
long looked for star, and announced its
return in some journal of the day. The
paragraph was widely copied throughout
the country. The idea pleased the popu-
lar fancy, was received with almost un-
questioning faith. and the sky was eagerly
scanned for a glimpse of the star that
nee shone over the humble dwelling that
enshrined the Redeemer of mankind.
Even the peerless Venus was impressed
into service, and was firmly believed to
be the sacred star once more shining
upon the earth after wandering for ages
in the star depths.
The history of the SO called Star Of
Bethlehem is briefly this: Tycho Brahe,
a Danish astronomer, discovered, in the
year 1879, an apparently new star near
Caph in Cassiopea. When first seen, in
November, it had attained the first mag
nitude. 1t increased rapidly in brilliancy,
until it rivaled Venus, and was visible at
monday. 1t began to diminish in bright
ness in December, and continded to fade
away until the following May, when it
disappeared from view.
Forty years later, when the telescope
was invented, a small telescope sta was
found close to the spot where the WON
derful star was seen. 1t is still there,
and is probably the same. 1t is now
classed among variable stars, and is,
fhnrnfNrn hnh1A 81 I1--~ 1911
time in the same extraordinary manner.
After classifying the star as a variable,
the next thing to be lone was to find out
its period of variability. Astronomical
records were searched, and it was ascer-
tanned that about the years 1868 and $50
bright stars suddenly appeared near the
same quarter of the heavens. 1t was,
therefore, classified as a variable, with q
period of about 300 years. Counting
back three periods from 956, the exact
period being uncertain, the star may
have appeared near the time of the Chris
tan era. Some imaginative observer,
for this reason, christened it the Star of
Bethlehem, and with scarce the shadow
Of a foundation the name has adhered to
it ever since. 1t is also known as the
Pilgrim Star, and among astronomers az
the star of 1879.
If the star be a variable, with a period
approximating to 800 years, 1t is now
due and liable to burst forth into sudden
brllliancy at any time. No celestial event
would be more welcome to astronomers.
The scientific world would be wild with
excitement over the su~bstantiation of an
ingenious theory and the confirmation Of
its hopes. Its first appearance, its exact
position in the heavens, its changes from
day to day, would be telegraphed all over
the country and infinitely described in
the journals of the day. The advent of
a comet, spanning the sky from the
zenith to the horizon, would be of no ac-
count in comparison with the blazing
start Meantime the telescope star near
Caph in Cassiopea shows no signs of any
coming disturbance, and observers must
wait patiently for developments, remem-
bering that the outburst will be sudden,
if it come.
1t is generally considered that the ex-
traordinary changes of light in stars, like
that of 1912, are caused by sudden out
bursts of glowing hydrogen gas, which by
its own light and by heating up the whole
surface of the star causes the immense
increase IN brilliancy. The spots, facule
and rosy protuberances on the sun give
some idea, on a small scale, of what may
be going on in other suns on a much
larger scale. Fortunately, the pew or
temporary stars observed by terrestrial
astronomers number only about twenty
four, an infinitesimal number when COM
pared with the boundless millions Of stars
that shine with nearly unchanging bright
ness. The probability is, therefore, small
that our sun will be added to the list of
blazing stars. He will probably shine for
millions of years to come, as he has shone
for millions of years in the past, and if
observed from other suns and systems
will be classed as q variable, with a period
of about eleven years, corresponding to
he cycle of sun spots.-Scientiic Amer
lean.